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The Rotation of the Mars Planet

Published online by Cambridge University Press:  14 August 2015

N. Borderies  and
G. Balmino
N. Borderies
Affiliation:
Groupe de Recherches de Géodésie Spatiale - Toulouse - France
G. Balmino
Affiliation:
Groupe de Recherches de Géodésie Spatiale - Toulouse - France

Extract

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In a non-inertial reference frame, of which the motion is given, the differential equations describing the rotation of a planet around its center of mass can be derived either under the form of Euler type equations, or from certain relations between angular velocity vectors or even angles. Unfortunately these equations are not well adapted to an analytical integration. Nevertheless, with some simplifications, Ward (1973), and Christensen (1977), by considering the motion of the spin axis in a non-inertial reference frame attached to the moving orbital plane, have found very large periodic variations in the obliquity of the Mars planet over a period of the order 1.2 10+5 years, which would be of great importance to the climatic history of the planet.

Type
Part III: Ephemerides, Equinox and Occultations
Information
Symposium - International Astronomical Union , Volume 81: Dynamics of the Solar System , 1979 , pp. 145 - 150
Copyright
Copyright © Reidel 1979 

References

Borderies, N, 1977: Mutual gravitational Potential of N Solid Bodies Cel. Mech. in press.Google Scholar
Brouwer, D. and Van Woerkom, A.J.J., 1951 - Astron. Pap. Amer. Ephemeris Naut. Alm., Vol XIII, pt II, 81.Google Scholar
Ward, W.R.; 1973, Science, Vol. 181, pp. 260–262 Google Scholar
Christensen, E.J., 1977: Rotation of Mars, J.P.L., Report 9 00.796 Google Scholar